Constraining thawing and freezing models with cluster number counts

Abstract

Measurements of the cluster abundance as a function of mass and redshift provide an important cosmological test that probe not only the expansion rate but also the growth of perturbations. In this paper we adopt a scalar field scenario which admits both thawing and freezing solutions from an appropriate choice of the model parameters and derived all relevant expressions to calculate the mass function and the cluster number density. We discuss the ability of cluster observations to distinguish between these scalar field behaviors and the standard $\Lambda$CDM scenario by considering the eROSITA and SPT cluster surveys.

9 pages, 5 figures, LaTeX

References in corpus (12)

• Dynamics of dark energy
• Cosmology and the Fate of Dilatation Symmetry
• The halo mass function from the dark ages through the present day
• Structure formation in the presence of dark energy perturbations
• The Cluster Mass Function from Weak Gravitational Lensing
• Scalar-field-dominated cosmology with a transient accelerating phase
• Chasing the phantom: A closer look at Type Ia supernovae and the dark energy equation of state
• Confronting Dark Energy Models using Galaxy Cluster Number Counts
• The spherical collapse model and cluster formation beyond the $\Lambda$ cosmology: Indications for a clustered dark energy?
• Virialization of cosmological structures in models with time varying equation of state
• Lectures on Dark Energy and Cosmic Acceleration
• Cosmology with the largest galaxy cluster surveys: Going beyond Fisher matrix forecasts

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• Cosmological constraints on galaxy cluster structure
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